\begin{table}%ta.1
\caption{\label{tab:radial}Error-weighted radial velocity measurements for the targets listed in Table~\ref{tab:targets}$^{a, b}$.}
%\centerline
 {\small \begin{tabular}{lclccccccccl}
\hline\hline\noalign{\smallskip}
& & & Range$^{d}$ & \multicolumn{7}{c}{Modified julian date}  & \\
ID         &Epochs& Line(s)$^{c}$ & (km~s$^{-1}$)   & 54637 & 54646 & 54665 & 54671 & 54692 & 54695 & 54713 & Notes \\
\hline
W2a        &  5   & Pa11-16, He~I &$-51.0$ -- $-14.1$ & --      & $-49.3$ & $-56.2$ & $-33.9$ & $-54.1$ & --      & $-18.6$ & Cand. binary\\ 
W8b        &  5   & Pa11-16       &$-61.6$ -- $-40.3$ & --      & $-61.6$ & $-49.9$ & $-40.3$ & $-47.4$ & --      & $-50.7$ & \\ 
W21        &  5   & Pa11-14       &$-57.4$ -- $-31.1$ & --      & $-57.4$ & $-35.0$ & $-43.1$ & $-55.1$ & --      & $-31.1$ & \\ 
W23a       &  5   & Pa11-16       &$-62.4$ -- $-42.9$ & --      & $-47.9$ & $-55.6$ & $-56.6$ & $-42.9$ & --      & $-62.4$ & \\ 
W43a       &  5   & Pa11-14       &$-137.9$ -- $+8.1$ & --      &$-109.7$ &$-123.1$ & $+8.1$  & $-38.8$ & --      &$-137.9$ & Binary\\
W55$^{e}$  &  7   & Pa11-14       &                   & $-43.1$ & $-49.9$ & $-55.4$ & $-45.4$ & $-43.8$ & $-53.9$ & $-55.5$ & \\
W60$^{e}$  &  5   & Pa11-14       &                   & --      & $-40.5$ & $-48.3$ & $-45.8$ & $-48.2$ & --      & $-37.7$ & \\
W71        &  7   & Pa11-16, He~I &$-61.9$ -- $-38.7$ & $-57.3$ & $-52.9$ & $-39.4$ & $-47.3$ & $-44.8$ & $-46.4$ & $-62.4$ & \\
W78        &  5   & Pa11-15       &                   & --      & $-46.7$ & $-46.4$ & $-41.3$ & $-39.9$ & --      & $-49.5$ & Puls. BSG \\
W84        &  5   & Pa11-13       &                   & --      & $-53.8$ & $-59.0$ & $-54.9$ & $-54.6$ & --      & $-55.8$ & \\                                 
W234$^{e}$ &  7   & Pa11-13       &$-67.0$ -- $-30.8$ & $-67.0$ & $-66.9$ & $-66.2$ & $-30.8$ & $-46.4$ & $-56.9$ & $-32.7$ & Prob. binary \\                               
W239$^{f}$ &  5   & C~III~$\lambda$8664 & $-81.6$ -- $+14.1$ & -- & $-26.9$ & $-10.7$ & $+14.1$ & $-49.7$ & --    & $-81.6$ & Wolf-Rayet\\
W243$^{g}$ &  5   & N~I (1 \& 8)  &$-28.8$ -- $-20.4$ & --      & $-22.7$ & $-20.4$ & $-27.7$ & $-28.3$ & --      & $-28.8$ & Puls. LBV \\
W265$^{g}$ &  5   & N~I (1 \& 8)  & N/A$^{h}$         & --      & $-47.6$ & $-36.8$ & $-36.0$ & $-37.9$ & --      & $-49.8$ & Puls. YHG \\
W373$^{e}$ &  5   & Pa11-14       &                   & --      & $-50.8$ & $-50.9$ & $-45.8$ & $-53.8$ & --      & $-52.9$ & \\
W3002$^{e}$&  5   & Pa11-14       &                   & --      & $-36.1$ & $-38.6$ & $-47.7$ & $-39.4$ & --      & $-43.0$ & \\
W3003$^{e}$&  5   & Pa11-14       &$-54.6$ -- $-4.4$  & --      & $-4.4$  & $-43.7$ & $-54.6$ & $-22.0$ & --      & $-10.6$ & Prob. binary\\
W3004$^{e}$&  5   & Pa11-14       &$-62.3$ -- $-35.5$ & --      & $-47.9$ & $-62.3$ & $-54.3$ & $-35.5$ & --      & $-46.0$ & \\
W3005$^{e}$&  5   & Pa11-13       &                   & --      & $-43.9$ & $-46.9$ & $-52.4$ & $-51.6$ & --      & $-49.9$ & \\
\hline
\end{tabular}}
\medskip
$^{a}$ Errors are not listed, but are $\le$4~km~s$^{-1}$ for the OB supergiants, $\le$3~km~s$^{-1}$ for the two cool hypergiants and $\lesssim$10~km~s$^{-1}$ for the Wolf-Rayet \object{W239}; $^{b}$~the broad, weak Paschen-series absorption lines in \object{W30a} precluded accurate RV measurement, while RV measurements for the eclipsing binary \object{W13} discussed in Sect.~\ref{sec:w13}
will appear in a forthcoming paper; $^{c}$~the line(s) used for RV measurement; $^{d}$~the range of measured radial velocities is given for targets in which statistically-significant variations are detected; $^{e}$~displays a distorted Pa-16 line due to blending with C~III$\lambda$8500 and a weak Pa-15 line that yield discrepant radial velocities 
compared to the other Paschen-series lines; $^{f}$~the C~III~$\lambda$8500 and C~III~$\lambda$8664 lines seen in the spectrum of the Wolf-Rayet \object{W239} give  discrepant RV measurements ($\sim$25~km~s$^{-1}$; see discussion in Sect.~\ref{sec:w239}). The value for C~III~$\lambda$8664 is given here; $^{g}$~the cool hypergiants \object{W243} and \object{W265} display rich absorption-line spectra, with a large number of potential lines suitable for RV measurement. The values given here are the average of nine of the strongest unblended N~I absorption lines from multiplets~1 and~8 \citep{moore}. Note that in both objects species-to-species variation in RV is seen, with clear 
evidence of velocity stratification in the photosphere of \object{W265} (see discussion in text); $^{h}$ The range of observed radial velocities in \object{W265} varies depending on the absorption line used to make the measurement.  See Sect.~\ref{sec:hypergiants}.
\end{table}